Distribution and evolution of Li abundance in red clump stars can be explained by the internal gravity waves

Abstract

The study of Li phenomena in red clump (RC) stars can give us a deeper understanding of the structure and evolution of stars. \citet{2022ApJ...933...58C} explained the RC Li abundance distributions naturally using only standard post main sequence (MS) Li evolution models when the distribution of progenitor masses and the depletion of Li during the MS observed in MS stars were considered, thus neither extra Li depletion nor Li creation mechanism is required. Nevertheless, it is interesting to consider the effects of mixing caused by some extra mechanisms. By constructing different models, we find that the mixing caused by internal gravity waves can explain the observed Li abundances of RC stars with low mass progenitors. To explain that, we rely on the extra mixing induced by internal gravity waves that are excited at the bottom of the convective envelope at the red giant branch (RGB) stage. During the RGB stage, introducing the internal gravity waves can improve the diffusion coefficient and strengthen the mixing effect. The effective enrichment of Li occurs at the late RGB stage and requires the diffusion coefficient of H-burning shell to reach $\sim 10^8\mathrm{c}{\mathrm{m}}^2{\mathrm{s}}^{-1}$. Our models predict that the Li abundance decreases from $\sim 1.5\mathrm{dex}$ to $\sim 0.0\mathrm{dex}$ at the end of core He-burning stage, thereby revealing the $\sim 99\%$ of the observed Li abundance distribution. The thermohaline mixing regulates the Li abundance of RGB stars, which combines with the internal gravity waves can explain the Li abundances of most giants.

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Cited by in corpus (3)

• Convective Mixing: The Formation Channel of Li-rich Giants
• Mixing by Internal Gravity Waves in Stars: Assessing Numerical Simulations Against Theory
• Unevolved Li-rich stars at low metallicity: a possible formation pathway through novae